Upper limits on the central black hole masses of 47 Tuc and NGC 6397 from radio continuum emission

Rijcke, S. De; Buyle, Pieter; Dejonghe, Herwig

doi:10.1111/j.1745-3933.2006.00153.x

Cited by 28 publications

(23 citation statements)

References 37 publications

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“…Although it is believed that such objects should be formed in dense stellar systems such as GCs, the observational evidences for their existence had been elusive. For instance, based on the lack of electromagnetic counterparts in X-rays 64 and radio waves 65 , in the GC 47 Tucanae, which is at distance of ~4 kpc, upper limits of 470 and 2,060 M had been placed on the mass of a putative IMBH.…”

Section: Intermediate Mass Black Holes In Globular Clustersmentioning

confidence: 99%

The formation of stellar black holes

Mirabel

2017

New Astronomy Reviews

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Abstract:It is believed that stellar black holes (BHs) can be formed in two different ways: Either a massive star collapses directly into a BH without a supernova (SN) explosion, or an explosion occurs in a proto-neutron star, but the energy is too low to completely unbind the stellar envelope, and a large fraction of it falls back onto the short-lived neutron star (NS), leading to the delayed formation of a BH. Theoretical models set progenitor masses for BH formation by implosion, namely, by complete or almost complete collapse, but observational evidences have been elusive. Here are reviewed the observational insights on BHs formed by implosion without large natal kicks from: (1) the kinematics in three dimensions of space of five Galactic BH X-ray binaries (BH-XRBs), (2) the diversity of optical and infrared observations of massive stars that collapse in the dark, with no luminous SN explosions, possibly leading to the formation of BHs, and (3) the sources of gravitational waves produced by mergers of stellar BHs so far detected with LIGO. Multiple indications of BH formation without ejection of a significant amount of matter and with no natal kicks obtained from these different areas of observational astrophysics, and the recent observational confirmation of the expected dependence of BH formation on metallicity and redshift, are qualitatively consistent with the high merger rates of binary black holes (BBHs) inferred from the first detections with LIGO.

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Section: Intermediate Mass Black Holes In Globular Clustersmentioning

confidence: 99%

The formation of stellar black holes

Mirabel

2017

New Astronomy Reviews

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“…Another possibility for detection would be radio emission from Bondi accretion of ambient material from the ISM [305]. Several studies used this method to place upper limits on the possible mass of IMBHs in Galactic globular clusters [98, 465, 32, 300] but there are no definitive detections. Indeed many studies are consistent with there being no IMBHs in the Galactic globular clusters (e.g., [311, 312].…”

Section: Dynamical Evolutionmentioning

confidence: 99%

Relativistic Binaries in Globular Clusters

Benacquista¹,

Downing

2013

Living Rev. Relativ.

198

129

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Galactic globular clusters are old, dense star systems typically containing 104–106 stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution that leads to relativistic binaries, and current and possible future observational evidence for this population. Our discussion of globular cluster evolution will focus on the processes that boost the production of tight binary systems and the subsequent interaction of these binaries that can alter the properties of both bodies and can lead to exotic objects. Direct N-body integrations and Fokker-Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.

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“…The masses of the putative black holes in the cores of well-known globular clusters such as 47 Tuc and NGC 6397, are expected to be ∼(10 2 -10 3 ) M (De Rijcke et al 2006). ULXs are observed in both spiral and elliptical galaxies, i.e.…”

Section: Introductionmentioning

confidence: 99%

On the evolution and fate of super-massive stars

Yungelson

Heuvel²,

Vink

et al. 2007

A&A

108

114

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Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60-1000 M . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aims. We predict the outcomes of stellar evolution by employing a mass-loss prescription that is consistent with the observed Hertzsprung-Russell Diagram location of the most massive stars. Methods. We compute a series of stellar models with an appropriately modified version of the Eggleton evolutionary code. Results. We find that super-massive stars with initial masses up to 1000 M end their lives as objects less massive than 150 M . These objects are expected to collapse into black holes (with M < ∼ 70 M ) or explode as pair-instability supernovae. Conclusions. We argue that if ultraluminous X-ray sources (ULXs) contain intermediate-mass black holes, these are unlikely to be the result of runaway stellar collisions in the cores of young clusters.

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Upper limits on the central black hole masses of 47 Tuc and NGC 6397 from radio continuum emission

Cited by 28 publications

References 37 publications

The formation of stellar black holes

The formation of stellar black holes

Relativistic Binaries in Globular Clusters

On the evolution and fate of super-massive stars

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